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The GJ 436 planetary system is an extraordinary system. The Neptune-sizeplanet that orbits the M3 dwarf revealed in the Ly$\alpha$ line an extendedneutral hydrogen atmosphere. This material fills a comet-like tail thatobscures the stellar disc for more than 10 hours after the planetary transit.Here, we carry out a series of 3D radiation hydrodynamic simulations to modelthe interaction of the stellar wind with the escaping planetary atmosphere.With these models, we seek to reproduce the $\sim56\%$ absorption found inLy$\alpha$ transits, simultaneously with the lack of absorption in H$\alpha$transit. Varying the stellar wind strength and the EUV stellar luminosity, wesearch for a set of parameters that best fit the observational data. Based onLy$\alpha$ observations, we found a stellar wind velocity at the position ofthe planet to be around [250-460] km s$^{-1}$ with a temperature of$[3-4]\times10^5$ K. The stellar and planetary mass loss rates are found to be$2\times 10^{-15}$ M$_\odot$ yr$^{-1}$ and $\sim[6-10]\times10^9$ g s$^{-1}$,respectively, for a stellar EUV luminosity of $[0.8-1.6]\times10^{27}$ ergs$^{-1}$. For the parameters explored in our simulations, none of our modelspresent any significant absorption in the H$\alpha$ line in agreement with theobservations.

GJ 436b and the stellar wind interaction: simulations constraints using Ly$\alpha$ and H$\alpha$ transits